Figures REF  and REF  show 4\(^{\prime \prime }\)  \(\times \)  4 \(^{\prime \prime }\)  HST \(F775W\)  cutout images, 4\(^{\prime \prime }\)  \(\times \)  4\(^{\prime \prime }\)  cutouts of the HST segmentation map, the target's continuum-component masks (in the spatial resolution of MUSE, 15\(^{\prime \prime }\)  \(\times \)  15\(^{\prime \prime }\) ), and the neighboring object masks (in the spatial resolution of MUSE, 15\(^{\prime \prime }\)  \(\times \)  15 \(^{\prime \prime }\) ), respectively. We used the HST segmentation map in [1]} following [2]}, which indicates areas in which galaxies are detected and defines the boundaries of the objects. The segmentation map was created with Source Extractor [3]} with multiple thresholds for detection and deblending, in order to deblend sources and optimize detections and photometries, as no single set of such thresholds perfectly detects bright, faint, large, and small sources simultaneously (see Section 3.5 and Table 2 in [1]}). They had four iterations. The parameter set for the first iteration is called “Deep” with detect_thresh=1.1\(\sigma \) and detect_minarea=9, with which source definitions near bright targets were poorly defined. The second “Shallow” run has detect_thresh=3.5\(\sigma \) and gave better detections for bright sources. They merged the two catalogs into one, but both runs have difficulty in deblending sources. Then, they had two more iterations called “Deep Deblend” and “Shallow Deblend”, which are with normal deblending parameters and lower deblending thresholds (see their Table 2). The resulting catalogs are merged into a single catalog with a single segmentation map [1]}.
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